The paper introduces the updated version of the PARSEC stellar evolution code, which includes significant revisions to input physics and the addition of the pre-main sequence (PMS) phase. The code now allows for the generation of accurate opacity tables consistent with any selected initial chemical composition by coupling OPAL opacity data at high temperatures with molecular opacities computed using the $\mathbb{E}$SOPUS code. The authors present extended sets of stellar evolutionary models for various initial chemical compositions, with a focus on solar-like metallicities and a wide range of initial masses from 0.1 to 12 solar masses. They also derive isochrones in several photometric systems to provide tools for modeling star clusters and galaxies through population synthesis techniques. Key aspects of the input physics, including the solar distribution of heavy elements, opacity calculations, and nuclear reaction rates, are detailed. The paper discusses the calibration of model parameters using solar data and the effects of microscopic diffusion and convective overshoot on stellar evolution. The results include detailed evolutionary tracks and isochrones, which are available for a variety of initial chemical compositions and metallicities.The paper introduces the updated version of the PARSEC stellar evolution code, which includes significant revisions to input physics and the addition of the pre-main sequence (PMS) phase. The code now allows for the generation of accurate opacity tables consistent with any selected initial chemical composition by coupling OPAL opacity data at high temperatures with molecular opacities computed using the $\mathbb{E}$SOPUS code. The authors present extended sets of stellar evolutionary models for various initial chemical compositions, with a focus on solar-like metallicities and a wide range of initial masses from 0.1 to 12 solar masses. They also derive isochrones in several photometric systems to provide tools for modeling star clusters and galaxies through population synthesis techniques. Key aspects of the input physics, including the solar distribution of heavy elements, opacity calculations, and nuclear reaction rates, are detailed. The paper discusses the calibration of model parameters using solar data and the effects of microscopic diffusion and convective overshoot on stellar evolution. The results include detailed evolutionary tracks and isochrones, which are available for a variety of initial chemical compositions and metallicities.